We present visible and near-IR photometry and spectra of the type IIn supernova PSN J13522411.
The light curve indicates a peak < 50 days after discovery around M = 􀀀17, followed by a slow
decline. Spectra show strong hydrogen and helium emission that peaks 200 d after discovery, with
a P-Cygni pro le that becomes more absorptive as time progresses. We determine that the CSM is
in the form of a slow, dense stellar wind that has remained steady for 30 years. The low velocity of
the wind, 70 km/s, implies that the progenitor was probably a red or yellow supergiant. From the
light curve, we estimate the total radiated energy to be 1050 erg. Further details of the explosion
will be determined as time allows.

We present visible and near-IR photometry and spectra of the type IIn supernova PSN J13522411.
The light curve indicates a peak < 50 days after discovery around M = 􀀀17, followed by a slow
decline. Spectra show strong hydrogen and helium emission that peaks 200 d after discovery, with
a P-Cygni pro le that becomes more absorptive as time progresses. We determine that the CSM is
in the form of a slow, dense stellar wind that has remained steady for 30 years. The low velocity of
the wind, 70 km/s, implies that the progenitor was probably a red or yellow supergiant. From the
light curve, we estimate the total radiated energy to be 1050 erg. Further details of the explosion
will be determined as time allows.

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dc.type

text

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dc.type

Electronic Thesis

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thesis.degree.name

B.S.

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thesis.degree.level

Bachelors

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thesis.degree.discipline

Honors College

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thesis.degree.discipline

Physics

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thesis.degree.grantor

University of Arizona

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dc.contributor.advisor

Smith, Nathan

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